Figure 2

Animation associated with Figure 2 in "Neural Networks as Surrogate Solvers for Time-Dependent Accretion Disk Dynamics"by Shunyuan Mao, Weiqi Wang, Sifan Wang, Ruobing Dong, Lu Lu, Kwang Yi, Paris Perdikaris, Andrea Isella, Sébastien Fabbro, and Lile Wang. ApJ Letters, in press.<br><br>Comparison of surface density ($\Sigma$) predicted by the PINN (middle column) and simulated by FARGO3D (left column) for the fiducial case with a mass ratio $M_{\rm 2}/M_{\rm 1} = 10^{-3}$. The right column shows the difference between FARGO3D and PINN predictions (FARGO3D minus PINN), with a different color scale than the top and middle rows to better highlight the discrepancies. The movie show snapshots from 0 to 10 orbits.